基于混合求解法的二维多段翼气动噪声特性分析

基于混合求解法,通过对声源区计算域进行分区,研究了二维多段翼不同部件对远场声压级的贡献,给出了声场分布和远场指向性,发现前缘缝翼噪声和主翼尾缘噪声对远场的贡献较小,襟翼后缘噪声的贡献在总声压级中占主导地位,是值得关注的噪声来源。     

SETI implications of gravitational assist via chaotic trajectories of binary objects

Extrapolating from the technique of gravitational assist via chaotic trajectories of binary objects, this paper considers how such techniques might be used in other systems. We examine which types of systems are the best candidates for harvesting gravitational energy for payload ejection. We also consider what signatures might be present in either the asteroid orbits or radiation of the central body if extraterrestrial intelligences were to use such techniques about these candidate systems.The simulation studies show that current technology cannot approach the sensitivity needed to detect either of these signals. Instead, we provide these results as guidance to studies in coming decades on patterns that may indicate the use of an asteroid ejection system.     

Low light intensity effects on the growth,photosynthetic characteristics,antioxidant capacity,yield and quality of wheat (Triticum aestivum L.) at different growth stages in BLSS

Minimizing energy consumption and maximizing crop productivity are major challenges to growing plants in Bioregenerative Life Support System (BLSS) for future long-term space mission. As a primary source of energy, light is one of the most important environmental factors for plant growth. The purpose of this study is to investigate the effects of low light intensity at different stages on growth, pigment composition, photosynthetic efficiency, biological production and antioxidant defence systems of wheat (Triticum aestivum L.) cultivars during ontogenesis. Experiments were divided into 3 intensity-controlled stages according to growth period (a total of 65 days): seedling stage (first 20 days), heading and flowering stage (middle 30 days) and grain filling stage (last 15 days). Initial light condition of the control was 420 μmol m⁻² s⁻¹ and the light intensity increased with the growth of wheat plants. The light intensities of group I and II at the first stage and the last stage were adjusted to the half level of the control respectively. For group III, the first and the last stage were both adjusted to half level of the control. During the middle 30 days, all treatments were kept the same intensity. The results indicated that low-light treatment at seedling stage, biomass, nutritional contents, components of inedible biomass and healthy index (including peroxidase (POD) activity, malondialdehyde (MDA) and proline content) of wheat plants have no significant difference to the control. Furthermore, unit kilojoule yield of group I reached 0.591 × 10⁻³ g/kJ and induced the highest energy efficiency. However, low-light treatment at grain filling stage affected the final production significantly.     

一种获取耀斑光变曲线的高精度,高分辨方法

一种获取耀斑光变曲线的高精度、高分辨方法栗志，周卫红（中国科学院云南天文台，昆明６５００１１）关键词太阳耀斑，光变曲线，测量方法太阳耀斑物理机制的研究，需要得到耀斑核的辐射的演化，在光学波段常用耀斑在单色光的辐射强度的时间变化曲线作为分析依据［１］．...     

复合材料飞机机身工装模具一体化设计及验证

针对RX1E复合材料轻型飞机一体成型、胶结连接为主的工艺特性,进行了工艺方案的总体设计,包括装配顺序的确定和装配工装基准的选择等。其次,进行了一体化工装的结构设计,细化了制件模具的成型方案和结构零件的定位夹紧形式。最后,重新进行了尾翼、阻力板等较小部件制造,对一体化工装的实际使用进行了验证,类比分析了工装模具一体化的方案在复合材料结构轻型飞机机身上的技术可行性和先进性。研究成果可为复合材料飞机工装提供设计思路和参考。     

空间目标视星等曲线仿真

人类航天活动日益频繁,空间目标种类和数量不断增多,识别未知空间目标的关键特征具有重要的科学价值。本文通过辅助图形软件建模分割,获取球体、圆锥体和圆柱体带法向量的面元坐标;基于卫星仿真工具包,得到了目标轨道及位置参数,并结合双向反射分布函数各向异性Phong 模型和四元数姿态更新模型,完成了地基观测条件下4种形状空间目标的视星等仿真。仿真结果表明,目标受空间位置、形状和姿态的影响程度不同,其光度曲线具有各自特点。球体由于形状完全中心对称,光度曲线主要受空间位置的影响;圆锥体、正方体、圆柱体光度曲线的波形受形状影响较大,曲线走向受位置影响较大,波动频率受姿态角速率影响较大。通过统计分析相关数据,可为后续空间目标位置、姿态和形状的反演提供先验模型。     

低轨航天器弹道系数估算及热层大气模型误差分析

利用低轨（LEO）航天器在轨期间两行轨道根数（TLEs）数据,结合经验大气密度模型NRLMSISE00,反演计算得到其在轨期间的弹道系数B’,以31年B’的平均值代替弹道系数真值,分别通过标准球形目标卫星对比以及物理参数基本相同的非球形目标卫星对比,对弹道系数真值进行了检验;利用不同外形目标卫星弹道系数在不同太阳活动周内的变化规律,结合太阳和地磁活动变化,估计经验大气密度模型的误差分布. 结果表明,利用反演弹道系数31年的平均值来代替真值,其在理论值的正常误差范围内;大气密度模型误差在210～526km高度范围内存在相同的变化趋势,且模型误差随高度增加而增大;在短周期内B’变化与太阳活动指数F_10.7存在反相关性;密度模型不能有效模拟2008年出现的大气密度异常低. 以上结果表明,经验大气密度模型结果需要修正,尤其是在太阳活动峰年和谷年,此外,磁暴期间模型误差的修正对卫星定轨和轨道预报等也具有重要意义.     

A Light Source System of Multi-star Simulator with Adjustable Background and Controllable Magnitude

A light source of multi-star simulator capable of background adjustment and magnitude control has been designed. Two integrating spheres are employed as the star-point light source and the background light source respectively. A beam splitter prism has been designed to serve as the beam combiner for the star-point and the background light sources, and a mathematical model has been constructed respectively to compute the light flux of the two integrating spheres. A magnitude testing system and a background testing system have been created using low-light illuminometer, luminance meter, and testing instruments to measure the star-point magnitude and the background luminance of the multi-star simulator. The test results suggest that the star-point magnitude is adjustable from 0 to +5m_v, with a simulation precision superior to ±0.026m_v. The maximum background luminance is 3.8×10⁵ cd·m^-2, and the minimum background luminance is 6.4×10^-2 cd·m^-2. The designed light source system can meet the requirements for simulating the stellar map with a sky background.     

Big Bang Nucleosynthesis and the Density of Baryons in the Universe

Now that extragalactic deuterium observations are being made, Big Bang Nucleosynthesis (BBN) is on the verge of undergoing a transformation. Previously, the emphasis was on demonstrating the concordance of the Big Bang Nucleosynthesis model with the abundances of the light isotopes extrapolated back to their primordial values using stellar and Galactic evolution theories. Once the primordial deuterium abundance is converged upon, the nature of the field will shift to using the much more precise primordial D/H to constrain the more flexible stellar and Galactic evolution models (although the question of potential systematic error in 4He abundance determinations remains open). The remarkable success of the theory to date in establishing the concordance has led to the very robust conclusion of BBN regarding the baryon density. The BBN constraints on the cosmological baryon density are reviewed and demonstrate that the bulk of the baryons are dark and also that the bulk of the matter in the universe is non-baryonic. Comparison of baryonic density arguments from Lyman- clouds, x-ray gas in clusters, and the microwave anisotropy are made and shown to be consistent with the BBN value.     

Electron coronal density irregularity\overline {n^2 } /(\bar n)^2 from measurements of K-coronal and lyman lines brightnesses

We propose a technique to derive the coronal density irregularity factor , wheren is the electron density. The absolute photometric comparison between the intensity of UV lines and the white-light K-coronal polarized brightness (pB) provides an unique constraint on the inhomogeneity of the corona. The ratio of the measured H I Lyman (Ly-) line intensity to the resonant-scattering dominated H I Lyman (Ly-) intensity can be used to extract the collisonal component of the Ly-. This component yields an estimate of . The quantity is then obtained from white-light K-coronal measurements. The use of lines of the same atomic species minimizes the effects due to outflow velocities (i.e., Doppler dimming), and reduces the errors introduced by the uncertainties in the ionization balance, the atomic parameters, and the solar abundances. The UVCS/SOHO unique capability of performing cotemporal and cospatial measurements of the Ly- and Ly- lines, and ofpB makes this instrument ideal for implementing this technique.